Here, we demonstrate the performance of the end-to-end pipeline briefly. We have run a 10-minute snapshot observation with the SKA-1 Low station layout located within \(\sim \) 2 km of the central stationThe latest SKA-1 layouts are available at https://astronomers.skatelescope.org/DOCUMENTS/. The sky-model used is a 21-cm map generated from ReionYuga and point source obtained from the 400 MHz uGMRT observation of the ELAIS-N1 field [1]}. The simulation was done for a 32 MHz bandwidth, spread over 64 frequency channels centered at 142 MHz (\(z\sim \) 9). These are the model visibilities, which we corrupt with 0.01% calibration error and position error of \(\sim \) 0.02" (0.01% of the PSF size). For most science cases of interest, a calibration error of\(\sim \) 10% is tolerable. However, it was shown in [2]}, [3]} that for sensitive observations targeting the EoR signal errors \(\gtrsim \) 0.05% cause the residual foregrounds override the target. Thus, following that work, the test case taken here has 0.01% calibration error introduced. For position errors, while [2]}, [3]} provide a tolerance threshold of \(\sim \) 0.1". But more detailed simulation of [6]} showed a tolerance of about \(\sim \)  a few arcseconds. However, the test case shown here considers an even lower position inaccuracy (which may be possible with the large baselines and sensitive design for the upcoming SKA). We obtain the residual visibility by subtracting the model from the corrupted ones (see Figure REF ) and calculate the spherically averaged PS from it. The results are shown in Figure REF . It is seen that for an error of 0.01% in gain calibration, or 0.01% in source position, the Hi power spectrum is recoverable.
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